[14] Consequently, the Chinese name for Beta Coronae Borealis itself is 貫索三 (Guàn Suǒ sān, English: the Third Star of Rope Binding).

[19] Antoine Labeyrie and his coworkers resolved the pair by speckle interferometry in 1973 and found that the two stars were separated by about 0.25 arcseconds; this work was published in 1974.

[24] Neubauer's 1944 work found a small variation in the radial velocity of Beta Coronae Borealis with a periodicity of 320 days, suggesting the presence of a third, lighter, body in the system.

This study also found very weak evidence for the presence of a companion with a shorter, 21-day, period, but the data was insufficient to draw a positive conclusion.

[25] The brighter component, Beta Coronae Borealis A, is a rapidly oscillating Ap star, with a period of 16.2 minutes.